The Dearth of Massive, Helium-Rich White Dwarfs in Young Open Star Clusters

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dc.creatorKalirai, Jasonjot Singh
dc.creatorRicher, Harvey B.
dc.creatorHansen, Brad M. S.
dc.creatorReitzel, David
dc.creatorRich, R. Michael
dc.date2004-09-07
dc.date2004-12-07
dc.date.accessioned2026-07-07T02:14:31Z
dc.date.available2026-07-07T02:14:31Z
dc.descriptionSpectra have been obtained of 21 white dwarfs (WDs) in the direction of the young, rich open star cluster NGC 2099. This represents an appreciable fraction (>30%) of the cluster's total WD population. The mean derived mass of the sample is 0.8 Msun - about 0.2 Msun larger than the mean seen among field WDs. A surprising result is that all of the NGC 2099 WDs have hydrogen-rich atmospheres (DAs) and none exhibit helium-rich ones (DBs), or any other spectral class. The number ratio in the field at the temperatures of the NGC 2099 WDs is DA/DB ~ 3.5. While the probability of seeing no DB WDs in NGC 2099 solely by chance is ~2%, if we include WDs in other open clusters of similar age it then becomes highly unlikely that the dearth of DB WDs in young open clusters is just a statistical fluctuation. We explore possible reasons for the lack of DBs in these clusters and conclude that the most promising scenario for the DA/DB number ratio discrepancy in young clusters is that hot, high-mass WDs do not develop large enough helium convection zones to allow helium to be brought to the surface and turn a hydrogen-rich WD into a helium-rich one.
dc.description4 pages including 1 figure and 1 table, accepted in ApJ Letters. References added and discussion expanded in Section 5
dc.identifierhttps://arxiv.org/abs/astro-ph/0409172
dc.identifierhttp://arxiv.org/abs/astro-ph/0409172
dc.identifierAstrophys.J. 618 (2004) L129-L132
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/8141
dc.subjectAstrophysics
dc.titleThe Dearth of Massive, Helium-Rich White Dwarfs in Young Open Star Clusters
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